The planetary mass-total luminosity relation during the formation phase for hot gas accretion, analogous to Fig. 2. The lines in the panel at 3 Myr differ from the ones in Fig. 2, while those at 5 and 10 Myr are identical. Compared to the cold-nominal population there are three differences that are particularly well visible in the panel at 3 Myr: (1) no split in an accreting and evolving sequence, (2) at a given mass, for accreting planets, the highest luminosities are lower, and (3) a temporally later beginning of D-burning. Furthermore, the luminosities of planets that are no more accreting are still more luminous in the hot population than in the cold-nominal population (which are already high because of the core-mass effect) especially for planets with masses between ~5 M_♃ and the deuterium burning limit.